000056292 001__ 56292
000056292 005__ 20210121114525.0
000056292 0247_ $$2doi$$a10.1007/s10569-015-9644-1
000056292 0248_ $$2sideral$$a92242
000056292 037__ $$aART-2015-92242
000056292 041__ $$aeng
000056292 100__ $$0(orcid)0000-0002-7620-4523$$aCasanova, D.
000056292 245__ $$aLong-term evolution of space debris under the J2 effect, the solar radiation pressure and the solar and lunar perturbations
000056292 260__ $$c2015
000056292 5060_ $$aAccess copy available to the general public$$fUnrestricted
000056292 5203_ $$aThe aim of this paper is the development of a model to propagate space debris in the geostationary ring considering the J2 effect due to the Earth oblateness, the Sun and Moon perturbations, and the solar radiation pressure. We justify the importance of considering the J2 effect when propagating space debris independently of the ratio A / m for short and long-term propagation. We study the role of the Sun and the Moon in the period and amplitude of the inclination for different values of A / m. Thanks to the Hamiltonian formulation of the problem and the use of Poincaré’s variables it is possible to express the evolution of the space debris through a simplified dynamical system. We test and validate our obtained analytical solutions with the numerical ones, computed with a powerful integrator named NIMASTEP. We analyse the improvements obtained when we include the J2 effect and the third body perturbations by a rigorous comparison with a previous model, which only considers the solar radiation pressure. Finally, we study the effect of the area-to-mass ratio on short and long-term propagation.
000056292 536__ $$9info:eu-repo/grantAgreement/ES/UZ/CUD-1315$$9info:eu-repo/grantAgreement/ES/MINECO/2013-44217-R
000056292 540__ $$9info:eu-repo/semantics/openAccess$$aby-nc$$uhttp://creativecommons.org/licenses/by-nc/3.0/es/
000056292 590__ $$a1.594$$b2015
000056292 591__ $$aMATHEMATICS, INTERDISCIPLINARY APPLICATIONS$$b34 / 101 = 0.337$$c2015$$dQ2$$eT2
000056292 591__ $$aASTRONOMY & ASTROPHYSICS$$b37 / 62 = 0.597$$c2015$$dQ3$$eT2
000056292 592__ $$a1.025$$b2015
000056292 593__ $$aModeling and Simulation$$c2015$$dQ1
000056292 593__ $$aMathematical Physics$$c2015$$dQ1
000056292 593__ $$aSpace and Planetary Science$$c2015$$dQ2
000056292 593__ $$aAstronomy and Astrophysics$$c2015$$dQ2
000056292 593__ $$aApplied Mathematics$$c2015$$dQ2
000056292 593__ $$aComputational Mathematics$$c2015$$dQ2
000056292 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/acceptedVersion
000056292 700__ $$aPetit, A.
000056292 700__ $$aLemaître, A.
000056292 773__ $$g123, 2 (2015), 223-238$$pCelest. mech. dyn. astron.$$tCelestial Mechanics and Dynamical Astronomy$$x0923-2958
000056292 8564_ $$s2410507$$uhttps://zaguan.unizar.es/record/56292/files/texto_completo.pdf$$yPostprint
000056292 8564_ $$s59487$$uhttps://zaguan.unizar.es/record/56292/files/texto_completo.jpg?subformat=icon$$xicon$$yPostprint
000056292 909CO $$ooai:zaguan.unizar.es:56292$$particulos$$pdriver
000056292 951__ $$a2021-01-21-11:06:06
000056292 980__ $$aARTICLE